1 / 18

Detecting Neutrino Transients with optical Follow-up Observations

Detecting Neutrino Transients with optical Follow-up Observations. Marek Kowalski Humboldt-University, Berlin TeV-III Venice , 2007. Gravitative collaps of a very massive, rotating star (>25 M  ):. Simulation: MacFadyen (2000). Testing the Supernovae-GRB connection. Observation:

cruz
Download Presentation

Detecting Neutrino Transients with optical Follow-up Observations

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. Detecting Neutrino Transients with optical Follow-up Observations Marek KowalskiHumboldt-University, BerlinTeV-III Venice, 2007

  2. Gravitative collaps of a very massive, rotating star (>25 M): Simulation: MacFadyen (2000) Testing the Supernovae-GRB connection Observation: Rate of GRBs is just ~1% of SNe Ib/c. Question: Could there be mildly relativistic jets ( of a few) inside many SNe? GRBs Neutrinos could provide the answer: SN @ 10 Mpc: 30 neutrino events in a cube-kilometer detector! Ando & Beacom, PRL (2005); Razzaque, Meszaros & Waxman, PRL (2005). SNe ?

  3. SNe Dt=10 s Constraints on Quantum Gravity  Energy (TeV) Jacob, Piran 2006

  4. Optical Neutrino Follow-up IceCube

  5. Optical Neutrino Follow-up optical detection network of optical telescopes IceCube Neutrino-Trigger IceCube

  6. GRB / Supernova identification Supernova lightcurves Search for transient sources: • Supernova (rising lightcurve) Strizinger et al. (2003)

  7. GRB / Supernova identification GRB afterglows Search for transient sources: • Supernova (rising lightcurve) • Gamma-Ray Burst (afterglow) • Gamma-Dark Bursts (orphan afterglows) F ~ t-1.2 10 minutes 100 seconds Time of explosion: Kahn et al., 2006

  8. GRB / Supernova identification Time of explosion: MK, A. Mohr, 2007

  9. single neutrinos 2o x 2o 250 nm a day For IceCube 100 seconds Neutrino burst trigger IceCube pointing Doublet background rate: doublets Kappes et al., 2007 Background rate of 5 per year, but Field-of-View of 2o x 2o needed.

  10. others • Robonet-1.0 3 x 2.0 m FoV: 0.1 x 0.1 follow-up of ROTSE Global network of robotic telescopes • ROTSE III 4 x 0.45 m FoV: 1.9 x 1.9 rapid follow-up

  11. Correlating every neutrino (~105/a)? Mirror Area X Field of View

  12. Next generation of Wide-Field-Imagers: full sky coverage of the optical sky with 3-7 day cadence. Correlating every neutrino (~105/a)? Offline correlation of every neutrino will be possible! Mirror Area X Field of View

  13. Supernova sensitivity Ando & Beacom PRL2005 Sensitivity can be doubled by optical follow-up! MK, A. Mohr, 2007

  14. Conclusion • An observation proposed using neutrinos to trigger follow-up observations (see also talk by M. Tluzykont) • Significant sensitivity improvement for SNe, and perhaps GRBs • For some cases it is the only way to identify the source • Robotic telescopes for follow-up observations exist and are ready

  15. Can we observe all SNe within a certain distance and do the correlation with neutrinos offline? Galaxy data from HyperLeda, [Paturel et al. 2003 A&A,412, 45]

  16. Can we observe all SNe within a certain distance and do the correlation with neutrinos offline? Galaxy data from HyperLeda, [Paturel et al. 2003 A&A,412, 45] Galaxy B-band magnitude converted to SNe rate using type dependent conversion [Cappelaro 99]

  17. ~20th magnitude detection limit (1 m) ~0.003 background Distribution of Supernovae (simulation) Triple coincidence Ando & Beacom flux Rate [arbitrary unit] Double Coincidence Distance [Mpc]

  18. Optical Neutrino Follow-up

More Related